Angular momentum conservation in a simplified Venus General Circulation Model

Lee, C.; Richardson, M. I.

doi:10.1016/j.icarus.2012.10.007

Cited by 10 publications

(8 citation statements)

References 14 publications

(25 reference statements)

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“…In the literature, excellent AAM conservation properties have been reported in a model based on the spectral transform method [Lee and Richardson, 2012]. The CAM-SE and global spectral transform dynamical cores share some aspects such as colocation of prognostic variables (Arakawa A-grid staggering), make use of basis functions so derivative and integrals can be exactly computed (except for nonlinear terms), and the diffusion operators are higher order (typically forth order or higher).…”

Section: Summary and Discussionmentioning

confidence: 99%

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Held‐Suarez simulations with the Community Atmosphere Model Spectral Element (CAM‐SE) dynamical core: A global axial angular momentum analysis using Eulerian and floating Lagrangian vertical coordinates

Lauritzen

Bacmeister

Dubos

et al. 2014

J Adv Model Earth Syst

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In this paper, an analysis of the global AAM conservation properties of NCAR's Community Atmosphere Model Spectral Element (CAM-SE) dynamical core under Held-Suarez forcing is presented. It is shown that the spurious sources/sinks of AAM in CAM-SE are 3 orders of magnitude smaller than the parameterized (physical) sources/sinks. The effect on AAM conservation by changing various numerical aspects of the dynamical core (e.g., different vertical coordinates, reduced formal order of accuracy, increased dissipation, and decreased divergence damping) is investigated. In particular, it is noted that changing from Eulerian (hybrid-sigma) to floating Lagrangian vertical coordinates does not alter the global AAM conservation properties of CAM-SE.

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Section: Summary and Discussionmentioning

confidence: 99%

“…In particular, it was noted that the damping operators were very different between the dynamical cores. The superior performing model, in terms of credible atmospheric state, conserved AAM very well [ Lee and Richardson , ].…”

Section: Introductionmentioning

confidence: 99%

Held‐Suarez simulations with the Community Atmosphere Model Spectral Element (CAM‐SE) dynamical core: A global axial angular momentum analysis using Eulerian and floating Lagrangian vertical coordinates

Lauritzen

Bacmeister

Dubos

et al. 2014

J Adv Model Earth Syst

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“…Here, we aim to verify whether the total axial angular momentum reaches a steady-state within the context of our simulations (including all stabilizing measurements) and whether this steady-state axial angular momentum budget is maintained over the course of the simulation. The specific angular momentum l is given by (Lebonnois et al 2012;Lee & Richardson 2012):…”

Section: Appendix A: Stability and Model Steady-statementioning

confidence: 99%

Equatorial retrograde flow in WASP-43b elicited by deep wind jets?

Carone

Baeyens

Mollière

et al. 2020

Monthly Notices of the Royal Astronomical Society

151

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ABSTRACT We present WASP-43b climate simulations with deep wind jets (down to 700 bar) that are linked to retrograde (westward) flow at the equatorial day side for p < 0.1 bar. Retrograde flow inhibits efficient eastward heat transport and naturally explains the small hotspot shift and large day-night-side gradient of WASP-43b (Porb = Prot = 0.8135 d) observed with Spitzer. We find that deep wind jets are mainly associated with very fast rotations (Prot = Porb ≤ 1.5 d) which correspond to the Rhines length smaller than 2 planetary radii. We also diagnose wave activity that likely gives rise to deviations from superrotation. Further, we show that we can achieve full steady state in our climate simulations by imposing a deep forcing regime for p > 10 bar: convergence time-scale τconv = 106–108 s to a common adiabat, as well as linear drag at depth (p ≥ 200 bar), which mimics to first-order magnetic drag. Lower boundary stability and the deep forcing assumptions were also tested with climate simulations for HD 209458b (Porb = Prot = 3.5 d). HD 209458b simulations always show shallow wind jets (never deeper than 100 bar) and unperturbed superrotation. If we impose a fast rotation (Porb = Prot = 0.8135 d), also the HD 209458b-like simulation shows equatorial retrograde flow at the day side. We conclude that the placement of the lower boundary at p = 200 bar is justified for slow rotators like HD 209458b, but we suggest that it has to be placed deeper for fast-rotating, dense hot Jupiters (Porb ≤ 1.5 d) like WASP-43b. Our study highlights that the deep atmosphere may have a strong influence on the observable atmospheric flow in some hot Jupiters.

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“…This is due to the extreme sensitivity of the angular momentum budget. In particular, further studies have investigated the question of angular momentum conservation in the dynamical cores: showed the performances of the LMD Venus GCM (fair) and of the VenusCAM finite-volume core (poor), while Lee and Richardson (2012) investigated this conservation aspect for their spectral core, demonstrating an excellent degree of conservation. This angular momentum conservation and how it affects the overall budget may be partly responsible for the diversity seen in Figure 34.…”

Section: Main Issues In Venus Atmospheric Modelingmentioning

confidence: 99%